Hα Variability in PTFO8-8695 and the Possible Direct Detection of Emission from a 2 Million Year Old Evaporating Hot Jupiter

October 2016 • 2016ApJ...830...15J

Authors • Johns-Krull, Christopher M. • Prato, Lisa • McLane, Jacob N. • Ciardi, David R. • van Eyken, Julian C. • Chen, Wei • Stauffer, John R. • Beichman, Charles A. • Frazier, Sarah A. • Boden, Andrew F. • Morales-Calderón, Maria • Rebull, Luisa M.

Abstract • We use high time cadence, high spectral resolution optical observations to detect excess Hα emission from the 2-3 Myr old weak-lined T Tauri star PTFO 8-8695. This excess emission appears to move in velocity as expected if it were produced by the suspected planetary companion to this young star. The excess emission is not always present, but when it is, the predicted velocity motion is often observed. We have considered the possibility that the observed excess emission is produced by stellar activity (flares), accretion from a disk, or a planetary companion; we find the planetary companion to be the most likely explanation. If this is the case, the strength of the Hα line indicates that the emission comes from an extended volume around the planet, likely fed by mass loss from the planet which is expected to be overflowing its Roche lobe.


IPAC Authors


David Ciardi

Senior Scientist


Luisa Rebull

Senior Research Scientist


Julian van Eyken

Associate Scientist